Issue 
A&A
Volume 569, September 2014



Article Number  A3  
Number of page(s)  20  
Section  Planets and planetary systems  
DOI  https://doi.org/10.1051/00046361/201423567  
Published online  08 September 2014 
Rotational properties of the binary and nonbinary populations in the transNeptunian belt^{⋆,}^{⋆⋆}
^{1} Instituto de Astrofísica de Andalucía, CSIC, Apt 3004, 18080 Granada, Spain
email: thirouin@iaa.es
^{2} NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Received: 4 February 2014
Accepted: 26 June 2014
We present results for the shortterm variability of binary transNeptunian objects (BTNOs). We performed CCD photometric observations using the 3.58 m Telescopio Nazionale Galileo (TNG), the 1.5 m Sierra Nevada Observatory (OSN) telescope, and the 1.23 m Centro Astronómico Hispano Alemán (CAHA) telescope at Calar Alto Observatory. We present results based on five years of observations and report the shortterm variability of six BTNOs. Our sample contains three classical objects: (174567) 2003 MW_{12}, or Varda, (120347) 2004 SB_{60}, or Salacia, and 2002 VT_{130}; one detached disk object: (229762) 2007 UK_{126}; and two resonant objects: (341520) 2007 TY_{430} and (38628) 2000 EB_{173}, or Huya. For each target, possible rotational periods and/or photometric amplitudes are reported. We also derived some physical properties from their light curves, such as density, primary and secondary sizes, and albedo. We compiled and analyzed a vast light curve database for TNOs including centaurs to determine the lightcurve amplitude and spin frequency distributions for the binary and nonbinary populations. The mean rotational periods, from the Maxwellian fits to the frequency distributions, are 8.63 ± 0.52 h for the entire sample, 8.37 ± 0.58 h for the sample without the binary population, and 10.11 ± 1.19 h for the binary population alone. Because the centaurs are collisionally more evolved, their rotational periods might not be so primordial. We computed a mean rotational period, from the Maxwellian fit, of 8.86 ± 0.58 h for the sample without the centaur population, and of 8.64 ± 0.67 h considering a sample without the binary and the centaur populations. According to this analysis, regular TNOs spin faster than binaries, which is compatible with the tidal interaction of the binaries. Finally, we examined possible formation models for several systems studied in this work and by our team in previous papers.
Key words: planetary systems / Kuiper belt: general / techniques: photometric
Appendix A is available in electronic form at http://www.aanda.org
Full Table 1 is only available at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsarc.ustrasbg.fr/vizbin/qcat?J/A+A/569/A3
© ESO, 2014
1. Introduction
As of December 2013, 78 binary/multiple systems^{1} have been identified in the transNeptunian belt. The majority of such systems have only one satellite, but two systems are known to have two companions, Haumea and 1999 TC_{36} (Brown et al. 2006; Benecchi et al. 2010), while the Pluto system consists of the Pluto/Charon binary accompanied by four relatively small satellites. This means that ~5% of the known transNeptunian objects (TNOs) have at least one companion. However, some estimations indicate that the proportion of these systems must be up to 20−25% (Noll et al. 2008).
The discovery of binary/multiple systems in the transNeptunian belt is subject to observational limitations. In fact, large telescopes, typically 4m class telescopes, are required to detect companion(s). The first binary TNO (BTNO; apart from Charon) was the nearequalsized companion of 1998 WW_{31} (Veillet et al. 2002). This detection was a serendipitous discovery using the 3.6 m Canada France Hawaii Telescope under excellent weather and seeing conditions. Several large groundbased surveys dedicated to the discovery of TNOs had some sensitivity for detecting (or not) binaries, such as the Deep Ecliptic Survey (DES; Millis et al. 2002; Elliot et al. 2005), the Deep Keck Search for Binary Kuiper Belt Objects (Schaller & Brown 2003), and the Canada France Ecliptic Plane Survey (CFEPS; Jones et al. 2006). Groundbased surveys have detected only a few binaries, and especially nearequalsized systems with a large separation between the components. The most prolific tool for detecting such systems is the Hubble Space Telescope (HST), which has a high rate of discoveries (Noll et al. 2008).
A binarity orbital study supplies a vast set of information, such as mass, density, albedo, size of each of the components of the system (under some assumptions), as well as important clues about formation and evolution of the transNeptunian belt (Noll et al. 2008). Some approaches can be used to complement the binarity study, such as spectroscopy (Carry et al. 2011), and photometric studies. The shortterm variability allows us to retrieve rotation periods from the photometric periodicities and also provides constraints on shape (or surface heterogeneity) by means of the lightcurve amplitude. Unfortunately, fewer than 30 BTNOs have a welldetermined rotational period. The sample is highly biased because the majority of BTNOs (and TNOs in general) observed are large and bright objects with high lightcurve variability and short rotational period (Thirouin et al. 2010, 2012). In this work, we increase the number of BTNOs whose shortterm variability has been studied. From performing CCD photometric observations using several telescopes in Spain during the past five years, we report six BTNO shortterm variability studies. From the light curve, we derived some physical characteristics, such as density constraints, albedo, and primary/satellite sizes. Part of this paper is dedicated to the rotational properties of the binary and nonbinary populations. We study several spin frequency distributions to pinpoint evidence of tidal effects between the components of multiple systems.
This paper is divided into six sections. In the next section, we describe the observations and the data set. Section 3 describes the reduction techniques we used to derive periods and photometric ranges. In Sect. 4, we summarize our main results for each target. In Sect. 5, we discuss our results and present a summary about binarity and nonbinarity in the transNeptunian belt. Finally, Sect. 6 is dedicated to our conclusions.
2. Observations
2.1. Runs and telescopes
We present data obtained with the 3.58 m Telescopio Nazionale Galileo (TNG), with the 1.5 m Sierra Nevada Observatory (OSN) telescope, and with the 1.23 m Centro Astronómico Hispano Alemán (CAHA) telescope at Calar Alto Observatory between 2009 and 2012.
The TNG is located at the Roque de los Muchachos Observatory (La Palma, Canary Islands, Spain). Images were obtained using the Device Optimized for the LOw RESolution instrument (DOLORES, or LRS). This device has a camera and a spectrograph installed at the Nasmyth B telescope focus. We observed in imaging mode with the R Johnson filter and a 2 × 2 binning mode. The camera is equipped with a 2048 × 2048 CCD with a pixel size of 13.5 μm. The field of view is 8.6′ × 8.6′ with a 0.252″/pix scale (pixel scale for a 1 × 1 binning).
The 1.5 m telescope is located at the Observatory of Sierra Nevada (OSN), at Loma de Dilar in the National Park of Sierra Nevada (Granada, Spain). Observations were carried out by means of a 2k × 2k CCD, with a total field of view of 7.8′ × 7.8′. We used a 2 × 2 binning mode, which changes the image scale to 0.46″/pixel.
The 1.23 m CAHA telescope at Calar Alto Observatory is located in the Sierra de Los Filabres (Almeria, Spain). Observations were carried out by means of a 4k × 4k CCD, with a total field of view of 21.5′ × 21.5′ (in a 1 × 1 binning) and a pixel scale of 15 μm. We observed with the R Johnson filter and a 2 × 2 binning mode.
2.2. Observing strategy
Exposure times were chosen by considering two main factors: i) exposure time had to be long enough to achieve a signaltonoise ratio (S/N) sufficient to study the observed object (typically, S/N> 20); ii) exposure time had to be short enough to avoid elongated images of the target (telescope tracked at sidereal speed) or elongated field stars (telescope tracked at the object rate of motion). We always chose to track the telescope at sidereal speed. The drift rates of TNOs are low, typically ~2″/h, so exposure times around 400 to 700 s were used.
Observations at the OSN were performed without filter to maximize the S/N. As the main goal of our study is shortterm variability via relative photometry, the use of unfiltered images without absolute calibration is not a problem. The R Johnson filter was used during our observations with the TNG and with the 1.23 m CAHA telescope. This filter was chosen to maximize the object S/N and to minimize the fringing that appears at longer wavelengths in these instruments.
In this work, we focused on six BTNOs: Salacia, Varda, 2002 VT_{130}, 2007 UK_{126}, 2007 TY_{430}, and Huya. All relevant geometric information about the observed objects at the dates of observations, and the number of images and filters used are summarized in Table A.1.
3. Data reduction and analysis
3.1. Data reduction
During all observing nights, series of biases and flatfields were obtained to correct the images. Median bias and median flatfield frames were created for each observational night. Care was taken not to use bias and/or flatfield frames that might be affected by observational and/or acquisition problems. The median flatfields were assembled from twilightdithered images, and the results were inspected for possible residuals from very bright saturated stars. Flatfield exposure times were always long enough to ensure that no shutter effect was present, so that a gradient or an artifact of some sort could be present in the corrected images. Each target image was biassubtracted and flatfielded using the median bias and median flatfield of the corresponding observing night.
Relative photometry using between 10 to 25 field stars was carried out by means of the Daophot routines (Stetson 1987). We rejected images in which the target was affected by a cosmicray hit or by a nearby star. Care was taken not to introduce spurious results due to faint background stars or galaxies in the aperture. We used a common reduction software for photometry data reduction of all the images, adjusting the details of the parameters to the specificity of each data set.
The choice of the aperture radius is crucial. The aperture has to be as small as possible to obtain the highest S/N by minimizing the sky contribution. But, on the other hand, the aperture has to be large enough to include most of the target flux. Generally, we repeated the measurement using a set of apertures with radii around the full width at half maximum. Various reference star sets were used to obtain the relative photometry of all the objects. Several stars had to be rejected from the analysis because they presented some variability. The aperture size and the reference stars used were the two main factors to consider the validity of our data reduction. The star set and aperture value that gave the lowest scatter in the photometry of the stars of similar brightness to the target and of the target was used for the final result. The final photometry of our targets was computed by taking the median of all the light curves obtained with respect to each reference star. By applying this technique, spurious results were eliminated and the dispersion of photometry was improved.
During all observational campaigns, we studied the same field of view, and therefore the same reference stars for each observed object. When we combined data from several observing runs, we normalized the photometry data to their average because we did not have absolute photometry that would have allowed us to link runs. By normalizing over the averages of several runs, we assume that a similar number of data points are in the upper and lower part of the curves. This may not be so if runs were only two or three nights long, which is not usually the case. We wish to emphasize that we normalized to the average of each run, not the average of each night.
3.2. Perioddetection methods and single/double peaked light curve
The timeseries photometry of each target was inspected for periodicities by means of the Lomb technique (Lomb 1976) as implemented in Press et al. (1992). We also checked our results with several other timeseries analysis techniques, such as the phase dispersion minimization (PDM; Stellingwerf 1978), and the CLEAN technique (Foster 1995). The method developped by Harris et al. (1989) and its improvement (Pravec et al. 1996) was also used (PravecHarris method).
Finally, to measure the full amplitude (or peaktopeak amplitude) of shortterm variability, a first or secondorder Fourier fit (depending on whether we considered a single or doublepeaked rotational periodicity) to the data was performed.
Fig. 1 Upper panel: assuming TNOs as triaxial ellipsoids, with axes a>b>c (rotating around the short axis c corresponding to the lowest energy state of rotation), we obtain two brightness maxima and two minima per rotation cycle (doublepeaked light curve) as illustrated in the curve. The maxima correspond to the largest crosssection of the object projected in the direction to the observer. Lower panel: if the TNO is a MacLaurin spheroid with an albedo variation on its surface, we obtained one maximum and one minimum per rotation cycle (singlepeaked light curve). Note that the ordinates are magnitudes, not brightness. 
One important point is to distinguish between single and doublepeaked light curves. Except for a poleon view of an object, in which no rotational variability can be observed, the observer will detect rotational variability for the rest of configurations of the spin axis. Assuming a triaxial ellipsoid (also known as Jacobi ellipsoid), we have to expect a light curve with two maxima and two minima, corresponding to a full rotation (Fig. 1, upper panel). However, if the object is spherical or oblate (also known as MacLaurin spheroid) without any albedo variation on its surface, we have to expect a flat light curve. If this spheroid presents albedo variation on its surface, we have to expect a light curve with one maximum and one minimum (i.e., a singlepeaked light curve). In real cases, we have combinations of shape effects and albedo variations. In many cases, when the lightcurve amplitude is (very) small, it is very difficult or impossible to distinguish whether a light curve is single or doublepeaked. Then we have to find a criterion to distinguish between shape and albedo effects.
In Thirouin et al. (2010) and Duffard et al. (2009), we proposed a threshold at 0.15 mag to distinguish whether a light curve is due to the albedo or due to the object shape. We know that this is a simplification because there may be elongated objects whose rotational variability is smaller than 0.15 mag simply because their rotation axes are viewed close to poleon from Earth. However, these probably are only a small fraction of all the objects with variability below 0.15 mag because statistically only very few objects have spin axes near the poleon orientation. Thirouin (2013) determined the best lightcurve amplitude limit for distinguishing between shape and albedodominated lighcurves (i.e., distinguishing between single and doublepeaked lighcurves). We tested three lightcurve amplitude (Δm) limits: i) a threshold at Δm = 0.10 mag, ii) at Δm = 0.15 mag, and iii) at Δm = 0.20 mag, to distinguish between single and doublepeaked light curves. For example, using the first threshold, we consider that light curves with an amplitude smaller than or equal to 0.10 mag are singlepeaked (i.e., equivalent to assuming that the lightcurve variation is due to albedo markings), and lighcurves with an amplitude higher than 0.10 mag are doublepeaked (i.e., equivalent to assuming that the lightcurve variation is due to the elongated shape of the body). This has a profound effect on the final spinperiod distribution. One of the main results of this study is that the best Maxwellian fit (with a significance level of 99%) is obtained for a distribution compiled assuming a threshold of 0.15 mag. Thus, it seems that this value is a good measurement of the typical variability caused by albedo. On the other hand, the highamplitude light curves of large TNOs, which we can clearly attribute to a triaxialellipsoid shape, can indicate that the typical magnitude of hemispheric albedo changes if we compare the two maxima or two minima in the doublepeaked light curves. This is because these objects are so large that they are in hydrostatic equilibrium, and therefore the differences in their maxima and minima can only come from albedo changes on their surfaces. The brightness differences for 2003 VS_{2} and Haumea are around 0.04 mag (Thirouin et al. 2010), for 2007 TY_{430} the difference is around 0.05 mag (this work), whereas for Varuna the greatest difference is 0.1 mag (Thirouin et al. 2010). This means that the hemispherically averaged albedo has variations of about 4 to 10%. We expect that the variability induced by surface marks is about 0.1 mag. In the asteroid case, albedo variations are usually responsible for light curve amplitudes between 0.1 mag and 0.2 mag (Magnusson 1991; Lupishko et al. 1983; Degewij et al. 1979). Here, we chose an intermediate value of 0.15 mag as the most reliable threshold above which we can be nearly confident that the variations are caused by shape effects. This value has been used by several investigators as the transition from low to medium variability (Sheppard et al. 2008). We must point out that distinguishing between shape and/or albedo contribution(s) in a light curve is not trivial at all, so a criterion must be used.
In Table 2, we indicate the preferred photometric period, which is the rotational period obtained from our data reduction. The preferred rotational period, which is the rotational period assuming our criterion, is also listed. For example, for 2007 TY_{430}, the data analysis suggested a photometric singlepeaked rotational period, but given that it shows an amplitude larger than 0.15 mag, the amplitude variation is probably caused by the shape of the object, therefore the doublepeaked rotational period as the true rotational period for this object is preferred.
3.3. Satellite contribution to the light curve
Because we are study binaries (no eclipsing nor contact binaries), one has to keep in mind a possible contribution of the satellite in the photometry (and in turn in the light curve). Neither of the two components of the system are resolved in our data, and the magnitude of the pair is measured.
For a wide system with a long orbital period and large separation between the two components, the satellite contribution to the light curve is negligible. For a very faint satellite, its light curve contribution is also negligible. But systems with a short orbital period (typically a few days) and a small separation between the two components requires more attention. Various systems in our sample have an orbital period of about five days. Our observational runs are, generally, one week long, which means that an entire (or nearly entire) orbital period is covered. Depending on the geometry of the system, mutual events between the primary and the satellite can be observed. With only a few fully known orbits, predicting mutual events is difficult. Only two systems (except for contact binaries) have undergone or are undergoing mutual events: PlutoCharon (Binzel & Hubbard 1997), and SilaNunam (Grundy et al. 2012; Benecchi et al. 2014). Five of the six systems studied in this paper do not have a fully known orbit, therefore we checked each observational night for possible mutual events between the primary and the satellite. No mutual event was detected during our shortterm variability runs.
4. Photometric results
In this section, we present the shortterm variability results that are summarized in Table 2. The light curves and Lomb periodograms for all objects are provided in Appendix A. We only present an example of a Lomb periodogram and a light curve in Figs. 2 and 3. We plotted all light curves over two cycles (rotational phase from 0 to 2) for a better visualization of the cyclical variation. Times for zero phase are reported in Table 2, without lighttime correction and at the beginning of the integration. For each light curve, a first or secondorder Fourier series is used to fit the photometric data. Error bars for the measurements are not shown in the plots for clarity, but onesigma error bars on the relative magnitudes are reported in the supplementary material (see Table 1). We must point out that when we combined several observing runs obtained at different epochs, lighttime correction of the data is required.
Timeseries photometry.
4.1. The system (174567) 2003 MW_{12} (or Varda) and Ilmarë
Using HST images obtained in April 26th 2009, the discovery of a satellite (Ilmarë) was reported in 2011 (Grundy et al. 2011a). Ilmarë is faint, with an apparent magnitude difference^{2} of ~1.45 mag in the F606W band^{3}.
Varda was observed in July 2009 and 2011 with the TNG, in June 2012 and in July 2013 at the OSN. The Lomb periodogram (Fig. A.1) shows several peaks. The highest peak with a significance level of 95% is located at 5.91 h (4.06 cycles/day) and the two 24 h aliases^{4} are at 7.87 h (3.04 cycles/day) and at 4.76 h (5.04 cycles/day). The first alias seems to have a higher confidence level than the second. All techniques (PDM, CLEAN, and PravecHarris method) inferred a rotational period of 5.91 h or 7.87 h. A 5.91 h rotational period is favored with a higher confidence level and therefore appears to be the best option. In Fig. A.2 we plot the corresponding singlepeaked light curve with an amplitude of 0.02 ± 0.01 mag. We must point out that for very low amplitude objects, it is difficult to estimate a secure rotational period. In fact, small variations in the nighttonight photometry can transmit more power to/from a 24 halias from/to the main peak. This means that we cannot completely discard the 7.87 h or the 4.76 h singlepeaked rotational period.
4.2. The system (120347) 2004 SB_{60} (or Salacia) and Actaea
Using HST images, Noll et al. (2006) reported the discovery of a satellite (named Actaea) with an apparent magnitude difference of about 2.36 mag in the F606W band.
Salacia was observed in July and October 2011 with the 3.58 m TNG, in September and October 2012, and in August 2013 at the OSN. The Lomb periodogram (Fig. A.3) shows one main peak with the highest spectral power (significance level of 99%) located at 3.69 cycles/day (6.5 h) and the one alias with a lower spectral power located at 2.71 cycles/day (8.86 h). All techniques inferred the spin period of 6.5 h with the highest spectral power. In Fig. A.4, the corresponding singlepeaked light curve with a peaktopeak amplitude of 0.06 ± 0.02 mag is plotted.
Summary of the results from this work and from the literature.
4.3. The system 2002 VT_{130}
Using HST images, Noll et al. (2009) announced the discovery of a satellite with an apparent magnitude difference of 0.44 mag in the F606W band. 2002 VT_{130} was observed during only one night in 2011 with the TNG. From about 4 h of observations, we report a 0.21 mag amplitude variation. We searched for a rotational periodicity but, unfortunately, with only few observational hours, we are not able to propose a reliable rotationalperiod estimation. To our knowledge, there is no bibliographic reference to compare our results with.
Fig. 2 Lombnormalized spectral power versus frequency in cycles/day for 2007 TY_{430}: the Lomb periodogram shows one main peak located at 4.64 h (5.17 cycles/day). 
Fig. 3 2007 TY_{430} light curve: rotational phase curves for 2007 TY_{430} obtained by using a spin period of 4.64 h (plot a)) and using a spin period of 9.28 h (plot b)). The continuous lines are a Fourier series fits of the photometric data. Different symbols correspond to different dates. The same legend is used in both plots. 
4.4. The system (229762) 2007 UK_{126}
Grundy et al. (2011a) reported the discovery of a companion with a magnitude difference of 3.79 mag in the F606W band.
2007 UK_{126} was observed on October 2011 with the TNG. We report three observational nights with a time base (time coverage between the first and the last image of the night) of about 4 h, ~4 h, and ~2 h, respectively. The Lomb periodogram (Fig. A.5) shows one main peak with a significance level of 95% located at 11.05 h (2.17 cycles/day), and several peaks located at 14.30 h (1.68 cycles/day) and at 20.25 h (1.19 cycles/day). All techniques confirmed these peaks, with a slight preference for the peak at 11.05 h. 2007 UK_{126} presents a nearly flat light curve with a photometric variation of 0.03 ± 0.01 mag (Fig. A.6). We must point out that the presence of numerous aliases with significant spectral power in the Lomb periodogram complicates the study and we are not able to propose a secure rotational period based on our data. We can only conclude that this object probably has a long rotational period (>8 h).
4.5. The system (341520) 2007 TY_{430}
From data acquired with the 8.1 m Gemini telescope (Hawaii, USA), Sheppard & Trujillo (2008) confirmed the presence of a satellite. The apparent magnitude difference is very low, ~0.1 mag (mean value) for this equalsized system (Sheppard et al. 2012).
2007 TY_{430} was observed during about 14 h, in four nights with the TNG in 2011. The Lomb periodogram (Fig. 2) shows one clear peak with a high confidence level (99%), located at 4.64 h (5.17 cycles/day). All techniques confirmed this periodicity. In Fig. 3, we present the singlepeaked light curve with a rotational period of 4.64 h and an amplitude of 0.20 ± 0.03 mag. The light curve amplitude is large, therefore, according to our definition (see Sect. 3.2), we have to consider the doublepeaked rotational period, 9.28 h, as true rotational period. The doublepeaked light curve has an amplitude peaktopeak of 0.24±0.05 mag (Fig. 3). We must point out that the first maximum is slightly taller than the second (~0.05 mag). This difference confirms the irregular shape of 2007 TY_{430} and clearly favors the doublepeaked light curve. However, we do not know if the variation comes from the primary or the satellite because both objects are apparently of very similar size which prevents us from distinguishing their contributions to the light curve.
4.6. The system (38628) 2000 EB_{173} (or Huya)
2000 EB_{173} (hereinafter Huya) is a resonant object and belongs to the plutino subcategory (i.e., it belongs to the 3:2 mean motion resonance with Neptune). From data acquired with the HST, Noll et al. (2012) confirmed the discovery of a satellite with an apparent magnitude difference around 1.4 mag in the F606W band.
Huya was observed in 2010, 2012, and 2013 with the 1.5 m OSN telescope and with the 1.23 m Calar Alto telescope. The Lomb periodogram (Fig. A.7) shows one peak with a high spectral power located at 5.28 h (4.55 cycles/day), and three aliases located at 6.63 h (3.62 cycles/day), at 4.31 h (5.57 cycles/day), and at 9.15 h (2.62 cycles/day). However, in all cases, these peaks have a lower spectral power than the main peak. All techniques confirm the highest peak at 5.28 h, and the aliases with a lower spectral power. In Fig. A.8, the corresponding singlepeaked light curve with an amplitude of 0.02 ± 0.01 mag is plotted. We must point out that the rotational period around 6 h noted by Ortiz et al. (2003a) is also a possibility in the newest data set, but as an alias. As already mentioned, for very low amplitude objects, it is difficult to estimate a secure rotational period estimation. In fact, small variations in the photometry can transmit more power to/from a 24 halias from/to the main peak. Therefore, we cannot discard the alias as a true period.
5. Discussion
In this section, we exhaustively study binarity in the transNeptunian belt. The main purpose is to determine if the binary and nonbinary populations share the same rotational features. Finally, we derive several physical properties and propose possible formation models for all binaries whose shortterm variability has been reported in this work and in Thirouin et al. (2010, 2012).
5.1. Derived properties from light curves of binary/multiple systems
The rotational properties of small bodies provide information about important physical properties, such as shape, density, and cohesion (Pravec & Harris 2000; Holsapple 2001, 2004; Thirouin et al. 2010, 2012). For binaries it is also possible to derive several physical parameters of the system components, such as diameters of the primary/secondary and albedo under some assumptions. Studying the shortterm variability of binary/multiple systems also allows us to identify which systems are tidally locked and which are not (Rabinowitz et al. 2013; Benecchi & Sheppard 2013).
In the next paragraph, we present the methodology for deriving the density, albedo, and primary/secondary sizes from the light curve. Then, we compare our results as well as our technique for deriving this information from the light curve with other methods. In fact, the density, albedo and/or sizes of both components can also be obtained from other methods, such: i) thermal or thermophysical modeling based on data obtained, for example, with the Herschel Space Observatory or the Spitzer Space Telescope (Müller et al. 2010; Stansberry et al. 2008); ii) from the mutual orbit of the binary component (Grundy et al. 2008; Brown et al. 2010); iii) from direct imaging (Brown & Trujillo 2004), or iv) from stellar occultation by (B)TNOs (Sicardy et al. 2011; BragaRibas et al. 2013). However, these methods only provide some information which requires the complement of other techniques. For example, thermal modeling, which provides the albedo and effective diameter of the system, requires the absolute magnitude as well as the rotational period of the object to derive reliable results (Müller et al. 2010; Lellouch et al. 2010; Lim et al. 2010; Vilenius et al. 2012). On the other hand, stellar occultations allow us to derive the size of the object with a high precision, but the system density can only be derived if the system mass is known (Sicardy et al. 2011). If the system mass is unknown (or if the object is not a binary), the lower limit of the density can only be estimated from the light curve (Ortiz et al. 2012a).
5.1.1. Density, size, and albedo from light curves: methodology
Assuming TNOs as triaxial ellipsoids, with axes a>b>c (rotating along c), the light curve amplitude, Δm, varies as a function of the observational (or aspect) angle ξ (angle between the rotation axis and the line of sight) according to Binzel et al. (1989): (1)The lower limit for the object elongation (a/b), assuming an equatorial view (ξ = 90°), is . According to the study of Chandrasekhar (1987) of equilibrium figures for fluid bodies, we can estimate lower limits for densities from rotational periods and the elongation of objects. That is to say, assuming that a given TNO is a triaxial ellipsoid in hydrostatic equilibrium (a Jacobi ellipsoid), we can compute a lower density limit. Based on this ρ, one can define the volume of the system as V_{system} = M_{system}/ρ, where M_{system} is the mass of the system and is known from the orbit of the system. We assume that both components have the same density, which is the system density. If the two components of the system have the same albedo, the primary radius (R_{primary}) can be expressed as (2)where Δ_{mag} is the component magnitude difference (Noll et al. 2008). Assuming that both components have the same albedo, the satellite radius is R_{satellite} = R_{primary}10^{− 0.2Δmag}.
We can derive the geometric albedo in the λ band, p_{λ}, given by the equation: (3)where C_{λ} is a constant depending on the wavelength (Harris 1998), and H_{λ} is the absolute magnitude in the λ band. The effective radius of the system, R_{effective}, is R_{effective} = . It is important to remember that we derived the lower limit of the density, so the derived sizes are upper limits and the derived albedo is a lower limit. We used the same method and the same assumptions to derive the density of Jacobi and MacLaurin objects.
5.1.2. Density, size, and albedo from light curves: results
In Table A.3, the density, primary and satellite sizes and albedo from light curves are summarized for each system studied in this work, in Thirouin et al. (2010), and in Thirouin et al. (2012). To estimate the sizes and the albedos using previous equations, we need the system masses that are summarized in Table A.3. From the light curves, we report albedo, primary/satellite sizes, and the lower limit of the density for seven systems. In three cases, we are only able to derive the lower limit of the density. For the system 2002 VT_{130}, we are not able to derive these parameters because we can only constrain its shortterm variability.
As already pointed out, lowamplitude light curves (Δm ≤ 0.15 mag) can be explained by albedo heterogeneity on the surface of a body that does not have a Jacobi shape, while largeamplitude light curves (Δm> 0.15 mag) are probably due to the shape of an elongated Jacobi body. In Table A.3, we reported a lower limit of the density computed following the study of Chandrasekhar (1987) of equilibrium figures for fluid bodies. To compute the lower limit of the density according to Chandrasekhar (1987), we have to assume that the object is a triaxial ellipsoid in hydrostatic equilibrium. This means that, according to our criterion, only objects with a largeamplitude light curve have to be considered as Jacobi ellipsoids. In our sample, only two binary systems have a largeamplitude light curve: 2007 TY_{430} and 2001 QY_{297}, and they can be considered as Jacobi ellipsoids. We found that the 2001 QY_{297} system has a very low lower density limit of 0.29 g cm^{3}, we derived a primary radius of <129 km, a secondary radius of <107 km, and a geometric albedo of >0.08 for the two components. For the system 2007 TY_{430}, we found that the two components have similar radii of <58 km (primary) and <55 km (secondary), we derived a lower limit to the density of 0.46 g cm^{3}, and a geometric albedo of >0.12 for both components. Most of the light curves of binary systems studied in this work and in Thirouin et al. (2010, 2012) are more significantly affected by albedo effects than by shape effects. In these cases, the objects are most likely spheroids, not Jacobi ellipsoids. As already pointed out, the lower limit of the density, and other parameters are only very crude estimate.
5.1.3. Density, size, and albedo from other methods
The component sizes and/or albedo can be estimated by other means. It is possible to verify whether the derived parameters from light curves and other methods are consistent or not, to check the validity of our method. In Table A.3, the density, the sizes of both components, and/or the albedo derived from other method(s) are summarized. As already mentioned, our method is only valid for Jacobi ellipsoids, therefore care has to be taken for objects with low variability, which are presumably MacLaurin spheroids. We must point out that for nonspherical bodies the concept of radius is unsuitable and we need to talk about an equivalent radius to that of a sphere in volume or in area. In conclusion, one must keep in mind that the radii proposed in Stansberry et al. (2008), Lellouch et al. (2010), Müller et al. (2010), Mommert et al. (2012), Vilenius et al. (2012), Fornasier et al. (2013), and Vilenius et al. (2014) are equivalent radii of the projected area, which means that densities should not be computed from these values.
For the systems QuaoarWeywot and OrcusVanth, our values are clearly unrealistic, but this was expected because in both cases, we studied MacLaurin spheroids. Based on the lowamplitude light curves of the systems SalaciaActaea, VardaIlmarë, and TyphonEchidna, we have to expect MacLaurin spheroids. For SalaciaActaea, we derived a density >1 g cm^{3}, a primary (secondary) radius of <491 km (<165 km), and a geometric albedo of >0.03 for the two components. Our albedo estimate is lower than the albedo obtained with thermal modeling, and we derived higher radii. For the systems VardaIlmarë and TyphonEchidna, we derived higher albedos and lower radii for the components. However, we must point out that our estimates for these three systems are consistent with the thermal modeling within the error bars. For 2007 TY_{430}, there is no study available to confirm our estimations. Sheppard et al. (2012) concluded that assuming a minimum density of 0.5 g cm^{3}, the system albedo is >0.17, and that of the radii of the two components are <60 km. This is similar to our own results, but they assumed a minimum density to start with. For the system 2001 QY_{297}, Vilenius et al. (2014) derived a density of 0.92 g cm^{3}, a geometric albedo of 0.075, and primary/secondary radii of about 85 km/77 km. For Huya, 2003 AZ_{84}, and 2007 UK_{126}, we only derived the lower density limits. However, because all of these systems have a lowamplitude light curve, our estimate can be unrealistic. In conclusion, deriving physical parameters such as albedo, sizes, and density from the light curves of binary systems is a reliable technique for Jacobi ellipsoids.
Fig. 4 Number of objects versus lightcurve amplitude: we consider three different samples: the whole sample (black bars), the sample without binary objects (gray bars), and the binary sample (white bars). 
5.2. Light curve amplitude and rotationalperiod distributions
Using the literature and the results presented in this work, we created a database of light curves with rotational periods and/or lightcurve amplitudes of binary/multiple systems. This database, updated on December 2013, is presented in Table A.2. We compiled 32 primaries and 3 satellites with a rotational period and/or peaktopeak amplitude or constraints^{5}.
5.2.1. Lightcurve amplitude distributions
The number of objects with a lightcurve amplitude value reported in the literature and in this work are reported in Figs. 4 and 5. Objects with only a constraint of their lightcurve amplitude were not taken into account.
In the Fig. 4 we focus on three samples: the entire sample, the binary population, and the sample without the binary population. First of all, we must point out that most objects (in the three samples) have an amplitude of <0.2 mag. About 57% of the entire sample, 59% of the sample without the binary population, and 54% of the binary sample have a low amplitude. The main reason for observing nearly flat light curves is probably a spherical object (or MacLaurin) with low albedo variations along the surface. The second option for this lightcurve amplitude can be an overabundance of nearly poleon orientation of the objects (rotational axis toward the observer). The most reasonable option is to consider that the observed objects are mostly MacLaurin spheroids with albedo marks with low contrast on their surfaces. Duffard et al. (2009) presented a model that used a Maxwellian rotational frequency distribution such as that obtained previously in this work, and assumed that the objects adopt hydrostatic equilibrium shapes. The model generates a set of 100 000 objects, and each object is randomly assigned to a rotation period from the distribution. All objects are assumed to be in hydrostatic equilibrium with a fixed density. The lightcurve amplitude is only a result of the shape of the body and the inclination of its rotation axis (randomly chosen). The body shapes are computed using Chandrasekhar (1987) equations. In other words, Jacobi ellipsoids produce a nonflat light curve, whereas MacLaurin spheroids generate a nearly flat light curve. One of the results of this model is that for a fixed density of 1 g cm^{3}, one expects 55.63% of MacLaurin spheroids and only 12.61% of Jacobi ellipsoids, while for a fixed density of 1.5 g cm^{3}, one expects 11.92% of Jacobi ellipsoids and 72.31% of MacLaurin spheroids. Because the centaurs are small and are not expected to be in hydrostatic equilibrium, and moreover, their rotations may be more evolved than those of the pure TNOs, we have removed them from the sample in Fig. 5.
Fig. 5 Number of objects versus lightcurve amplitude: we consider three different samples: the sample without the centaur population (black bars), the centaur population (gray bars), and the sample without the centaur and the binary populations (white bars). 
The sample without the binary and the centaur populations mainly has amplitudes between of 0.1 and 0.2 mag. In conclusion, there are hints that the binary amplitudes may be slightly larger than the nonbinary population, but overall the distributions are similar, and only more studies about the shortterm variability of binary systems will allow us to confirm or refute this tendency.
5.2.2. Rotational period distributions
Salo (1987) showed that asteroid rotation rates probably follow a Maxwellian distribution if the asteroids are in collisional equilibrium. Binzel et al. (1989) studied the asteroid rotation rate distributions and concluded that for asteroids with a diameter D> 125 km, a Maxwellian is able to fit the observed rotation rate distributions, implying that their rotation rates may be determined by collisional evolution. In contrast, for asteroids with a diameter D< 125 km, there is an excess of slow rotators and their nonMaxwellian distributions suggests that their rotation rates are more strongly influenced by other processes that result from their formation in catastrophic disruption events, etc. However, a recent study by Warner et al. (2009) suggested that the nonMaxwellian distribution for small main belt asteroids (MBAs) is mainly due to the Yarkovsky−O’Keefe−Radzievskii−Paddack (YORP, see Rubincam 2000 for more details) effect. Although TNOs are very different from asteroids, we can carried out a similar study. Because the number of TNOs/centaurs whose shortterm variability has been studied is still too limited, we did not divide the sample according to object sizes, and moreover, all TNOs studied here are larger than 125 km. As pointed out in Binzel et al. (1989), there are several biases in the asteroid light curve database, mainly because it is easier to determine reliable and publishable parameters for asteroids that have short rotational periods with a large lightcurve amplitude. Similar biases have been noted in the TNOs/centaurs light curve database (Sheppard et al. 2008; Thirouin et al. 2010). Binzel et al. (1989) tried to effectively eliminate bias effects by including all asteroids, even those with a low reliability code (a low reliability code means that the estimated rotational period has a low confidence level and may be incorrect). Binzel et al. (1989) stressed that excluding low reliability objects results in overweighting asteroids with large amplitudes and short periods, which introduces a significant bias in the results of the statistical studies. Based on such a study, we decided to proceed in the same way and included all TNOs/centaurs with a shortterm variability study, even if the rotational period estimated was not unambiguously determined. Finally, the bin size used here for the histograms is the same as that used in Binzel et al. (1989), mainly because the sample of TNOs/centaurs with a shortterm variability study is still too small to consider smaller bin sizes.
For multiple determinations of the period and/or amplitude, we selected the value preferred by the author(s) who published the study. If no preferred value was mentioned, we proceeded to a random choice. In some cases several rotational periods have been proposed for an object, for these we randomly chose one of these rotational periods. Either this, or one can simply give weights to each period according to the number of possible periods.
As in Binzel et al. (1989), we fitted the rotational frequency distribution to a Maxwellian distribution expressed as (4)where N is the number of objects, Ω is the rotation rate in cycles/day, σ is the width of the Maxwellian distribution. The mean value of this distribution is .
For many TNO light curves it is extremely difficult to distinguish whether the variability is due to albedo variations or an elongated shape. In other words, the derived rotational period have an uncertainty of a factor 2. In fact, a doublepeaked light curve is expected for a nonspherical object since the projected crosssection should have two minima and two maxima along one full object rotation. In contrast, light curves caused by albedo variations on the surface of the object are expected to be singlepeaked (see Lacerda & Luu 2003 for a complete review). Figure 6 was plotted considering that all objects (TNOs and centaurs) have i) singlepeaked light curves and ii) doublepeaked light curves. These are obviously extreme cases that are unrealistic. From Maxwellian fits to the rotational frequency distributions, the mean rotational periods are 5.35 ± 0.31 h for the entire sample assuming a singlepeaked rotation distribution, and 10.11 ± 0.59 h for the second distribution. Obviously, both distributions are unrealistic, but an upper limit to the rotational period distribution is provided assuming the double distribution. A more realistic distribution is to assume that all the light curves with an amplitude lower than 0.15 mag are singlepeaked (i.e., assuming that variability is due to albedo features), and light curves with a variability higher than 0.15 mag are doublepeaked (i.e., assuming that variability is due to the object’s elongated shape). In Fig. 7 we show such a distribution. Obviously, this criterion is a good first approximation, but some cases do not fit in it. For example, a doublepeaked rotational period of 5.92 h and a lightcurve amplitude of 0.09 mag have been reported for the Centaur Chiron (Bus et al. 1989). According to our criterion, a singlepeaked light curve has to be considered, but a rotational period of 2.96 h is quite unrealistic for this kind of object. In conclusion, in some cases it is necessary to decide on a casebycase basis.
In Fig. 7, three different samples are plotted: the entire sample, the binary population, and the sample without the binary population. From Maxwellian fits to the rotational frequency distributions, the mean rotational periods are 8.63 ± 0.52 h for the entire sample, 8.37 ± 0.58 h for the sample without the binary population and, finally, 10.11 ± 1.19 h for the binary population.
Duffard et al. (2009) noted that the centaur population has a higher mean rotational period. In fact, as this population is more collisionally evolved, their rotational periods might be affected. We removed them from our different samples and obtained two new Maxwellian distributions. In Fig. 8, we plot the sample without the centaur population and the sample without the centaur and the binary populations. Based on the Maxwellian distribution fits, we computed a mean rotational period of 8.86 ± 0.58 h, 8.64 ± 0.67 h for the sample without the centaur population and for the sample without centaur and the binary populations, respectively.
Fig. 6 Number of objects versus rotational rate in cycles/day: two different samples are plotted. Black bars: the entire sample considering that all the light curves are singlepeaked (number of objects (N) = 115). Gray bars: the entire sample considering doubleperiod light curves. A Maxwellian fit to the entire sample assuming a single period distribution gives a mean rotational period of 5.35 h (σ = 2.813 ± 0.262, continuous black line). The Maxwellian fit of the second sample gives a mean rotational period of 10.11 h (σ = 1.488 ± 0.139, continuous gray line). 
Fig. 7 Number of objects versus rotational rate in cycles/day: three different samples are plotted: the entire sample (number of objects (N) = 109, black bars), the binary population (N = 28, white bars), and the sample without the binary population (N = 81, gray bars). A Maxwellian fit to the entire sample gives a mean rotational period of 8.63 h (σ = 1.743 ± 0.167, continuous black line). The Maxwellian fit of the sample without binary objects gives a mean rotational period of 8.37 h (σ = 1.796 ± 0.199, continuous gray line). Finally, the fit for the binary population gives a mean rotational period of 10.11 h (σ = 1.487 ± 0.281, dashed black line). 
Fig. 8 Number of objects versus rotational rate in cycles/day: two different samples are plotted: the sample without the centaur population (number of objects (N) = 92, black bars), and the sample without the centaur and binary populations (N = 64, gray bars). A Maxwellian fit to the first sample gives a mean rotational period of 8.86 h (σ = 1.697 ± 0.177, continuous black line). The second Maxwellian fit of the sample without binaries nor centaurs gives a mean rotational period of 8.64 h (σ = 1.741 ± 0.217, continuous gray line). 
In conclusion, based on the Maxwellian distribution fits, we found a mean rotational period for the sample without the binary and the centaur populations of 8.64 ± 0.67 h, whereas the binary population seems to have a higher mean rotational period of 10.11 ± 1.19 h. This means that the binary systems rotate more slowly. We must point out that the number of binary/multiple systems whose shortterm variability has been studied is limited, but it is reasonable to expect that binary systems have longer rotational periodicities. In fact, tidal effects are able to slow down the primary (and the secondary) rotational rate (see Sect. 5.3).
5.3. Tidal effects
Tidal effects can synchronize the spin rate of the primary and/or of the secondary to its orbital period, and can circularize the satellite orbit.
5.3.1. Circularization time
According to Goldreich & Sari (2009), the tides raised on the primary are (5)where e is the orbital eccentricity, M_{satellite} and M_{primary} are the satellite and primary masses (respectively), a is the orbital semimajor axis, Q_{primary} is the dissipation parameter of the primary, R_{primary} is the primary radius, and n is the mean orbital angular velocity. The dissipation parameter depends on the body rigidity, the acceleration of gravity at the object surface, density, and size. According to Goldreich & Soter (1966), this parameter range is 10 to 6 × 10^{4}. The typical value used in the TNO case is Q = 100 (Noll et al. 2008). The Love parameter of the primary is (6)where g_{primary} = GM_{primary}/ is the surface gravity of the primary, ρ_{primary} is the primary density, and μ_{primary} is the primary rigidity. The rigidity is estimated to be 3 × 10^{10} N m^{2} for rocky objects and 4 × 10^{9} N m^{2} for icy ones (Gladman et al. 1996). In Table A.4, all the BTNOs whose shortterm variability was studied in this work, and in Thirouin et al. (2010, 2012) are reported, as well as the parameters needed to compute the circularization time. For Actaea, Ilmarë, and the satellite of Huya, the times required to circularize the orbit are short or similar to the age of the solar system, and therefore we expect nearly circular orbits. With an orbital eccentricity of 0.0084 ± 0.0076 and 0.02 ± 0.04 for Actaea and for Ilmarë (respectively), both orbits are nearly circular (Stansberry et al. 2012; Grundy et al. 2011b). The orbit of Huya’s satellite is unknown, but we have to expect a nearly circular orbit. The times required to circularize the orbit of Echidna and the satellite of 2007 UK_{126} are long, therefore we have to expect noncircular orbits. With an orbital eccentricity of 0.526 ± 0.015 for Echidna, its orbit is not circular (Grundy et al. 2008). The orbit of the satellite of 2007 UK_{126} is unknown, but we expect a noncircular orbit. The orbit of the satellite of 2007 TY_{430} is far from circular and will require a long time to be circular. According to Sheppard et al. (2012), the orbital eccentricity is 0.1529 ± 0.0028, which confirms the noncircular orbit. The orbits of Weywot and of the satellites of 2001 QY_{297} and 2003 AZ_{84} will also require a long time to be circular. Fraser et al. (2013) derived an orbital eccentricity of ~0.13−0.16 for Weywot, and Grundy et al. (2011b) estimated an orbital eccentricity of 0.4175 ± 0.0023 for the satellite of 2001 QY_{297}. This means that neither orbit is circular. The orbit of the satellite of 2003 AZ_{84} is unknown, but we expect a noncircular orbit. Based on the time required to circularize the orbit of Vanth, we can expect a noncircular orbit, which disagree with the upper limit of the eccentricity of 0.0036 estimated by Brown et al. (2010). But as pointed out in Ortiz et al. (2011), it is quite possible that Vanth has a much larger mass and size than originally estimated by Brown et al. (2010). However, not only the tidal effect may circularize the orbit, the Kozai mechanism can do this as well (Kozai 1962). Owing to the perturbation by the Sun, the orbit of the satellite experiences libration (oscillation) of its argument of pericenter. Porter & Grundy (2012) presented an exhaustive study about the Kozai effect on BTNOs. They simulated a large set of synthetic BTNOs and confirmed that the Kozai effect can completely reshape the initial orbits of the systems. According to the simulations of Porter & Grundy (2012), we have to expect many BTNOs with a very tight and circular orbits. To date, only 21 objects have wellknown orbits and 30 objects have ambiguous orbits, but apparently several systems have nearcircular orbits (Grundy et al. 2011a).
5.3.2. Synchronization time
Tidal effects can also synchronize the satellite and primary spin rates to the orbital period. Several formulas have been proposed in the literature to estimate the time needed to lock the primary/secondary rotational rates (Hubbard 1984; Gladman et al. 1996). Here, we compute such a time using the formula of Gladman et al. (1996) which takes into account the body rigidity. According to Gladman et al. (1996), the time needed (τ_{lock}) to tidally lock a primary is expressed as (7)where ω_{primary} is the initial rotational rate of the primary, a is the distance between the primary and the satellite, Q is the dissipation, G is the gravitational constant, M_{satellite} and R_{primary} are, respectively, the mass of the satellite and the radius of the primary, I is the moment of inertia of the primary (such as ), and k_{primary} is the Love number of the primary.
In Table A.4 we summarize the parameters used to compute the time needed to tidally lock the primary. We considered three cases: i) the density of the satellite is the same as the density of the primary (i.e., the system density); ii) the density of the satellite is 1 g cm^{3}, and iii) the density of the satellite is 0.5 g cm^{3}. Assuming a dissipation of Q = 100 and that both components have the same density, times to tidally lock most of the binaries presented here are long (compared with the age of the solar system), and so we have to expect that none of these systems is tidally locked. We must point out that this fact is confirmed thanks to our shortterm variability studies of these systems, which show evidence for rotation periods of several hours (see Thirouin et al. 2010, 2012, and this work). The times to tidally lock Huya and Varda are short. Therefore, we can expect that these systems can be tidally locked. However, there is evidence for rotation periods of several hours, and therefore primaries are not tidally locked (see Thirouin et al. 2010, 2012, and this work). By considering a satellite with a lower density (0.5 g cm^{3}) and a rigidity for rocky bodies, we computed times to tidally lock the primary at about 10^{9} years; a higher Q might also explain longer locking times. The computed tidal locking times according to Gladman et al. (1996) seem agree with our observational results. In conclusion, the systems studied here and in Thirouin et al. (2010, 2012) are not yet synchronous (or double synchronous). But the tidal effects between the primary and the satellite might already have slowed down the primary rotational rate and might explain the rotational period distributions. On the other hand, we must point out that tidal circularization and tidal despinning are complex effects. For example, for equalsize objects, the secondary tidal effect cannot be neglected. The assumptions used to derive Eq. (7) are not valid for binaries with a moderate to high eccentricity. More studies about tidal effects as well as estimations of the parameter Q are needed.
5.4. Formation of binary and multiple systems
Various models have been proposed to explain the formation of binary and multiple systems, such as the L^{3} mechanism by Goldreich et al. (2002), the L^{2}s mechanism by Goldreich et al. (2002), the chaosassisted capture by Astakhov et al. (2005), the collisional model by Durda et al. (2004), the hybrid model by Weidenschilling (2002), the gravitational collapse by Nesvorný et al. (2010), and the rotational fission model by Ortiz et al. (2012b). A complete review of some of these mechanisms can be found in Noll et al. (2008).
Both capture and collisional models require that the number of TNOs in the primordial transNeptunian belt was at least several orders of magnitude higher than currently and consequently, BTNOs are primordial systems (Petit & Mousis 2004). Only the formation of a few binary systems is well known, such as the Pluto/Charon formation. In fact, it is complicated to favor or discard any model, especially if the orbit is unknown. Currently, the binary formation via capture and/or collision as well as gravitational collapse are the most often investigated and seem the most probable in the transNeptunian belt. In fact, the rotational fission scenario is unlikely for most of the binaries, but in some cases it has to be considered (Ortiz et al. 2011, 2012b). One argument in favor of a rotational fission scenario for some cases is the specific angular momentum of a binary and multiple system. The specific angular momentum (SAM), computed according to Descamps & Marchis (2008) is (8)where q is the secondarytoprimary mass ratio, a is the semimajor axis, e is the eccentricity, and R_{primary} is the primary radius. The Ω parameter is the normalized spin rate expressed as , where ω_{primary} is the primary rotation rate and ω_{critical} the critical spin rate for a spherical body, such as , where G is the gravitational constant, M_{system} is the system mass and R_{effective} the effective radius of the system (or equivalent radius).
Assuming triaxial objects with semiaxes as a>b>c, the λ shape parameter is , where α = c/a and β = b/a. We considered the satellites to be spherical bodies, so λ_{satellite} = 1. The scaled spin rate (SSR), according to Chandrasekhar (1987), is expressed as, , where ρ_{primary} is the density of the primary. We considered that both components have the same density, which is the system density. The scaled spin rate and specific angular momentum are dimensionless values.
Fig. 9 Scaled spin rate versus specific angular momentum: scaled spin rate and specific angular momenta computed as mentioned in the text. We indicate the MacLaurin and the Jacobi sequences. The “high size ratio binaries”, as indicated in Descamps & Marchis (2008), are located near the MacLaurin/Jacobi transition. The legend is as follows: the black triangle denotes SalaciaActaea, the gray diamond HaumeaNamaka, the black diamond HaumeaHi’iaka, the gray triangle VardaIlmarë, the gray square QuaoarWeywot, the black circle OrcusVanth assuming a secondarytoprimary mass ratio of 0.03, the gray circle OrcusVanth assuming a secondarytoprimary mass ratio of 0.09, and black square for TyphonEchidna. The system 2007 TY_{430} is not plotted here because we restricted the plot for a better visualization). Error bars are approximate. 
Based on a binary asteroid population study, Descamps & Marchis (2008) concluded that binary systems near the MacLaurin/Jacobi transition are most likely formed by rotational fission or mass shedding. In Fig. 9 we indicate the MacLaurin and Jacobi sequences, the binary/multiple systems studied in this work, and those from Thirouin et al. (2010, 2012).
We computed a specific angular momentum of 0.36 ± 0.07 and a scaled spin rate of 0.49 ± 0.14 for the SalaciaActaea system. These values allow us to discard a rotational fission scenario to explain the formation of this system (Fig. 9). However, we must point out that several of the parameters used to compute the specific angular momentum and the scaled spin rate present a high uncertainty, and considering the error bars, SalaciaActaea may have suffered a rotational fission. For example, the SalaciaActaea system density presents a high uncertainty: i) 1.16 g cm^{3} according to Stansberry et al. (2012); ii) 1.38 ± 0.27 g cm^{3} according to Vilenius et al. (2012); and iii) 1.29 g cm^{3} according to Fornasier et al. (2013). The SalaciaActaea light curve is flat, and accordingly, this object presents a homogeneous shape little or no deformation. For this reason and because of the size of the satellite, a collisional scenario is not favored to explain the Actaea formation (except for a Pluto/Charon like formation). We suggest a capture or gravitational collapse model. A possible rotational fission scenario has to be confirmed.
We computed a specific angular momentum of 0.59 and a scaled spin rate of 0.61 for the VardaIlmarë system (Fig. 9). In this case, we did not compute the error bars^{6} of the specific angular momentum and the scaled spin rate, mainly because no density estimation is available for this system instead we used the lower limit of the density derived in this work, which, as already mentioned, is only a very crude estimation. The light curve of the VardaIlmarë system is flat. This means that this object is probably a MacLaurin spheroid (or near) with a limited shape deformation. Because of this, we favor a capture scenario or gravitational collapse instead of a collisional scenario to explain the satellite formation. The second argument to discard a collisional scenario is the size of the satellite. In fact, the large size of the satellite suggests a noncollisional formation, unless it was created in a similar Pluto/Charon formation model. We must mention that a flat light curve can be caused by a poleon orientation. In this case, the object may be deformed, but we cannot detect it in the lightcurve variation. However, we used the lower limit to the density to derive the specific angular momentum and the scaled spin rate, therefore we must keep in mind a possible rotational fission scenario to explain the formation of this system.
The wide binary 2007 TY_{430} with a specific angular momentum around 4.33 and a scaled spin rate around 0.61 is not plotted in Fig. 9 because it is out of the scale. To compute the specific angular momentum and the scaled spin rate of this system, we had to use the lower limit of the density derived in this work, which, as already mentioned, is only a very crude estimation. Sheppard et al. (2012) previously discussed in detail all possible (or impossible) formation models for this system. They considered two plausible scenarii: the L^{3} mechanism based on gravitational capture proposed by Goldreich et al. (2002), and the gravitational collapse mechanism studied by Nesvorný et al. (2010).
We computed a specific angular momentum of 0.15 ± 0.02 and a scaled spin rate of about 0.31 ± 0.12 for the QuaoarWeywot. This system does not seem to come from a rotational fission scenario (Fig. 9). The light curve of QuaoarWeywot has a moderate lightcurve amplitude. This means that this object is probably a MacLaurin spheroid (or near) with a limited shape deformation. However, the satellite, Weywot, has a small diameter of 81 ± 11 km according to Fornasier et al. (2013), and therefore a collisional scenario seems the best option to explain the satellite formation.
The specific angular momentum of 2001 QY_{297} is 1.85 ± 0.39 and its scaled spin rate is 0.58 ± 0.21, which is out of the scale in Fig. 9. These values seem to indicate that the 2001 QY_{297} binary system was not formed by rotational fission. In fact, the high value of the specific angular momentum and the scaled spin rate of this system do not fall into the “high size ratio binaries” region indicated in Fig. 9 of Descamps & Marchis (2008) and is far from the Jacobi or MacLaurin sequences. Accordingly, we can probably discard a possible rotational fission origin for this binary. We cannot favor any other formation scenario; this asynchronous binary could have been formed by capture and/or collision, or by gravitational collapse.
We computed a specific angular momentum of 0.73 ± 0.06 and a scaled spin rate of 0.66 ± 0.16 for TyphonEchidna. This is not too far from the high mass ratio binaries that most likely come from fissions. Therefore, we cannot discard rotational fission to explain the system (Fig. 9). The rotational period of the TyphonEchidna system is not secure, but we can affirm that the lightcurve amplitude is low. This means that this object is probably a MacLaurin spheroid with a limited shape deformation. We favor a capture scenario or gravitational collapse over a collisional scenario to explain the satellite formation. We must mention that flat light curve can be caused by a poleon orientation. In this case, the object may be deformed, but we cannot detect it in the lightcurve variation.
For OrcusVanth, we computed a specific angular momentum of 0.26 ± 0.02 and a scaled spin rate of 0.29 ± 0.06 considering a secondarytoprimary mass ratio of 0.03 (Brown et al. 2010), a specific angular momentum of 0.46 ± 0.02, and a scaled spin rate of 0.29 ± 0.06 (Ortiz et al. 2011), considering a secondarytoprimary mass ratio of 0.09 (Fig. 9). Ortiz et al. (2011) showed that the satellite rotation is synchronous (the rotational period of the satellite and the orbital period are the same), and that the system is not doublesynchronous because the primary is spining much faster than the orbital period (Thirouin et al. 2010). If we assume that the initial spin period of Orcus was approximately its critical value, the total angular momentum lost by the slowdown to 10 h would have been gained by the satellite, which would have reached exactly its current configuration if the mass ratio of the system was about 0.09 (the value obtained by assuming that the Vanth albedo is smaller than that of Orcus, which is probably the case judging from their very different spectra Carry et al. 2011). This would support the idea that the satellite might be the result of a rotational fission (Ortiz et al. 2011).
For Huya, we favor a capture scenario or a gravitational collapse because of the satellite size and the flat light curve. We propose a very flat light curve for 2007 UK_{126}, which seems to discard the collisional scenario. However, the size of the satellite is compatible with a collisional formation. In conclusion, we cannot favor or discard any formation model based on our study for this object. Based on only a few hours of observations, 2002 VT_{130} seems to have a high amplitude light curve which means that a collisional scenario may be an option. The system 2003 AZ_{84} is composed of a large primary and a small satellite. This means that a collisional scenario seems the best option.
6. Summary and conclusions
We have analyzed the shortterm variability of several binary transNeptunian objects (BTNOs). Only one object in our sample, 2007 TY_{430}, has a highamplitude light curve (Δm> 0.15 mag) and can be considered to be a Jacobi ellipsoid. Assuming that this system is in hydrostatic equilibrium, we derived a lower limit to the density (ρ> 0.46 g cm^{3}), a primary (secondary) radius of <58 (<55 km), and a geometric albedo of 0.12 for the two components. Other BTNOs studied in this work showed small peaktopeak amplitude variations and are oblate (MacLaurin spheroid). For them we were only able to derive mere academic guesses on density and geometric albedo. But we showed that deriving several parameters from the light curves is a reliable method for Jacobi ellipsoids.
An exhaustive study about shortterm variability as well as derived properties from light curves allowed us to draw some conclusions for the transNeptunian belt binary population. Based on Maxwellian fit distributions of the spin rate, we suggested that the binary population rotates slower than the nonbinary one. This slowingdown can be attributed to tidal effects between the satellite and the primary, as expected. We showed that no system in this work is tidally locked, but the primary despinning process may have already affected the primary rate (as well as the satellite rotational rate). We computed the time required to circularize and tidally lock the systems. We used the Gladman et al. (1996) formula to compute the time required to tidally lock the systems, but this formula is based on several assumptions and approximations that do not always hold. The computed times are reasonable in most cases and confirm that none of the systems is tidally locked, assuming that the satellite densities are low (≲0.5 g cm^{3}) and have a high rigidity or have a Q> 100 (higher dissipation than usually assumed). However, more studies are necessary to understand the tidal effect between primary and satellite, especially for equalsize systems.
Finally, by studying the specific angular momentum of the sample, we proposed possible formation models for several BTNOs with shortterm variability. In several cases, we obtained hints of the formation mechanism from the angular momentum, but for other cases we do not have enough information about the systems to favor or discard a formation model.
The exact definition of binarity is the following: a system composed of two objects orbiting their common center of mass or barycenter, which lies outside either body. For example, in the transNeptunian belt, the PlutoCharon system is a true binary. For most of the binary/multiple systems in this belt we have no information about their barycenter, so the use of this term has to be considered carefully. Often, the term binary/multiple is used to refer to systems with one or more companions despite the definition mentioned here.
A recent study of 2010 WG_{9} suggested a rotational period of 131.89 ± 0.06 h or 263.78 ± 0.12 h (Rabinowitz et al. 2013). Such long rotational periods have been observed only for tidally evolved BTNOs, suggesting that this object may be such a system. However, as the binarity of this object is not confirmed yet, we did not include it in our study.
In Fig. 9, we use an error bar of ±0.1 for the specific angular momentum and the scaled spin rate.
Acknowledgments
We thank the referee for his or her careful reading of this paper. We are grateful to the Sierra Nevada Observatory, Telescopio Nazionale Galileo and CAHA staffs. This research was based on data obtained at the Observatorio de Sierra Nevada, which is operated by the Instituto de Astrofísica de Andalucía, CSIC. Other results were obtained at the Telescopio Nazionale Galileo. The Telescopio Nazionale Galileo (TNG) is operated by the Fundación Galileo Galilei of the Italian Istituto Nazionale di Astrofisica (INAF) on the island of La Palma in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This research is also based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the MaxPlanck Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). A. Thirouin, N. Morales, and J. L. Ortiz were supported by AYA200806202C0301, and AYA201130106C0201, which are two Spanish MICINN/MEC projects. A. Thirouin, N. Morales, and J. L. Ortiz also acknowledge the Proyecto de Excelencia de la Junta de Andalucía, J.A.2007FQM2998. FEDER funds are also acknowledged.
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Online material
Appendix A
Fig. A.1 Lombnormalized spectral power versus frequency in cycles/day for Varda: the Lomb periodogram of our data sets shows that one highest peak is located at 5.91 h (4.06 cycles/day) and the two largest aliases are at 7.87 h (3.04 cycles/day) and at 4.76 h (5.04 cycles/day). 
Fig. A.2 Varda light curve: rotational phase curve for Varda obtained by using a spin period of 5.91 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 
Fig. A.3 Lombnormalized spectral power versus frequency in cycles/day for Salacia: the Lomb periodogram shows one main peak located at 3.69 cycles/day (6.5 h) and one alias at 2.71 cycles/day (8.86 h). 
Fig. A.4 Salacia light curve: rotational phase curve for Salacia obtained by using a spin period of 6.5 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 
Fig. A.5 Lombnormalized spectral power versus frequency in cycles/day for 2007 UK_{126}: the Lomb periodogram shows one peak with the highest spectral power located at 11.04 h (2.17 cycles/day), and several aliases located at 14.30 h (1.68 cycles/day) and at 20.25 h (1.19 cycles/day). 
Fig. A.6 2007 UK_{126} light curve: rotational phase curve for 2007 UK_{126} obtained by using a spin period of 11.05 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 
Fig. A.7 Lombnormalized spectral power versus frequency in cycles/day for Huya: the Lomb periodogram shows one main peak located at 5.28 h (4.55 cycles/day), and three aliases located at 6.63 h (3.62 cycles/day), at 4.31 h (5.57 cycles/day), and at 9.15 h (2.62 cycles/day). 
Fig. A.8 Huya light curve: rotational phase curve for Huya obtained by using a spin period of 5.28 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 
Dates (UTdates, format MM/DD/YYYY), heliocentric (r_{h}), and geocentric (Δ) distances, and phase angle (α).
Shortterm variability of BTNOs.
Density, size, and albedo from this work and from the literature.
System names, Love number of the primary (k_{primary}), primary and satellite densities (ρ_{primary} and ρ_{satellite}), initial rotational rate of the primary (T_{0}), mean orbital angular velocity (n), and orbital semimajor axis (a).
System names, secondarytoprimary mass ratio (q), semimajor axis (a), eccentricity (e), primary radius (R_{p}), rotational period of the primary and its critical rotational period (P_{p}, and P_{c}), and the λ shape parameter of the primary (λ_{p}) and satellite.
All Tables
Dates (UTdates, format MM/DD/YYYY), heliocentric (r_{h}), and geocentric (Δ) distances, and phase angle (α).
System names, Love number of the primary (k_{primary}), primary and satellite densities (ρ_{primary} and ρ_{satellite}), initial rotational rate of the primary (T_{0}), mean orbital angular velocity (n), and orbital semimajor axis (a).
System names, secondarytoprimary mass ratio (q), semimajor axis (a), eccentricity (e), primary radius (R_{p}), rotational period of the primary and its critical rotational period (P_{p}, and P_{c}), and the λ shape parameter of the primary (λ_{p}) and satellite.
All Figures
Fig. 1 Upper panel: assuming TNOs as triaxial ellipsoids, with axes a>b>c (rotating around the short axis c corresponding to the lowest energy state of rotation), we obtain two brightness maxima and two minima per rotation cycle (doublepeaked light curve) as illustrated in the curve. The maxima correspond to the largest crosssection of the object projected in the direction to the observer. Lower panel: if the TNO is a MacLaurin spheroid with an albedo variation on its surface, we obtained one maximum and one minimum per rotation cycle (singlepeaked light curve). Note that the ordinates are magnitudes, not brightness. 

In the text 
Fig. 2 Lombnormalized spectral power versus frequency in cycles/day for 2007 TY_{430}: the Lomb periodogram shows one main peak located at 4.64 h (5.17 cycles/day). 

In the text 
Fig. 3 2007 TY_{430} light curve: rotational phase curves for 2007 TY_{430} obtained by using a spin period of 4.64 h (plot a)) and using a spin period of 9.28 h (plot b)). The continuous lines are a Fourier series fits of the photometric data. Different symbols correspond to different dates. The same legend is used in both plots. 

In the text 
Fig. 4 Number of objects versus lightcurve amplitude: we consider three different samples: the whole sample (black bars), the sample without binary objects (gray bars), and the binary sample (white bars). 

In the text 
Fig. 5 Number of objects versus lightcurve amplitude: we consider three different samples: the sample without the centaur population (black bars), the centaur population (gray bars), and the sample without the centaur and the binary populations (white bars). 

In the text 
Fig. 6 Number of objects versus rotational rate in cycles/day: two different samples are plotted. Black bars: the entire sample considering that all the light curves are singlepeaked (number of objects (N) = 115). Gray bars: the entire sample considering doubleperiod light curves. A Maxwellian fit to the entire sample assuming a single period distribution gives a mean rotational period of 5.35 h (σ = 2.813 ± 0.262, continuous black line). The Maxwellian fit of the second sample gives a mean rotational period of 10.11 h (σ = 1.488 ± 0.139, continuous gray line). 

In the text 
Fig. 7 Number of objects versus rotational rate in cycles/day: three different samples are plotted: the entire sample (number of objects (N) = 109, black bars), the binary population (N = 28, white bars), and the sample without the binary population (N = 81, gray bars). A Maxwellian fit to the entire sample gives a mean rotational period of 8.63 h (σ = 1.743 ± 0.167, continuous black line). The Maxwellian fit of the sample without binary objects gives a mean rotational period of 8.37 h (σ = 1.796 ± 0.199, continuous gray line). Finally, the fit for the binary population gives a mean rotational period of 10.11 h (σ = 1.487 ± 0.281, dashed black line). 

In the text 
Fig. 8 Number of objects versus rotational rate in cycles/day: two different samples are plotted: the sample without the centaur population (number of objects (N) = 92, black bars), and the sample without the centaur and binary populations (N = 64, gray bars). A Maxwellian fit to the first sample gives a mean rotational period of 8.86 h (σ = 1.697 ± 0.177, continuous black line). The second Maxwellian fit of the sample without binaries nor centaurs gives a mean rotational period of 8.64 h (σ = 1.741 ± 0.217, continuous gray line). 

In the text 
Fig. 9 Scaled spin rate versus specific angular momentum: scaled spin rate and specific angular momenta computed as mentioned in the text. We indicate the MacLaurin and the Jacobi sequences. The “high size ratio binaries”, as indicated in Descamps & Marchis (2008), are located near the MacLaurin/Jacobi transition. The legend is as follows: the black triangle denotes SalaciaActaea, the gray diamond HaumeaNamaka, the black diamond HaumeaHi’iaka, the gray triangle VardaIlmarë, the gray square QuaoarWeywot, the black circle OrcusVanth assuming a secondarytoprimary mass ratio of 0.03, the gray circle OrcusVanth assuming a secondarytoprimary mass ratio of 0.09, and black square for TyphonEchidna. The system 2007 TY_{430} is not plotted here because we restricted the plot for a better visualization). Error bars are approximate. 

In the text 
Fig. A.1 Lombnormalized spectral power versus frequency in cycles/day for Varda: the Lomb periodogram of our data sets shows that one highest peak is located at 5.91 h (4.06 cycles/day) and the two largest aliases are at 7.87 h (3.04 cycles/day) and at 4.76 h (5.04 cycles/day). 

In the text 
Fig. A.2 Varda light curve: rotational phase curve for Varda obtained by using a spin period of 5.91 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 

In the text 
Fig. A.3 Lombnormalized spectral power versus frequency in cycles/day for Salacia: the Lomb periodogram shows one main peak located at 3.69 cycles/day (6.5 h) and one alias at 2.71 cycles/day (8.86 h). 

In the text 
Fig. A.4 Salacia light curve: rotational phase curve for Salacia obtained by using a spin period of 6.5 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 

In the text 
Fig. A.5 Lombnormalized spectral power versus frequency in cycles/day for 2007 UK_{126}: the Lomb periodogram shows one peak with the highest spectral power located at 11.04 h (2.17 cycles/day), and several aliases located at 14.30 h (1.68 cycles/day) and at 20.25 h (1.19 cycles/day). 

In the text 
Fig. A.6 2007 UK_{126} light curve: rotational phase curve for 2007 UK_{126} obtained by using a spin period of 11.05 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 

In the text 
Fig. A.7 Lombnormalized spectral power versus frequency in cycles/day for Huya: the Lomb periodogram shows one main peak located at 5.28 h (4.55 cycles/day), and three aliases located at 6.63 h (3.62 cycles/day), at 4.31 h (5.57 cycles/day), and at 9.15 h (2.62 cycles/day). 

In the text 
Fig. A.8 Huya light curve: rotational phase curve for Huya obtained by using a spin period of 5.28 h. The continuous line is a Fourier series fit of the photometric data. Different symbols correspond to different dates. 

In the text 
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